1. Local ULIRGs and Quasars S. Veilleux (U. Maryland)  AGN activity  Host Properties  Environments  Galactic Winds Three Pagodas, Dali, China (8/15/05) Real Observed

2. Ground-based Optical Spectroscopy  Fraction of Seyfert nuclei: ~ 5 % @ log[L IR /L Sun ] = 10 – 11 ~ 50% @ log[L IR /L Sun ] > 12.3 (SV et al. 1995; Kim, SV, & Sanders 1998; SV, Kim, & Sanders 1999; also Kewley, Dopita et al.) log(L IR /L Sun ) < 11 11 – 11.99 12 – 12.29 12.3 – 12.8 Total = 29 68 77 31

3. Ground-based vs HST/STIS (Farrah, Surace, SV, Sanders, & Vacca 2005) Ground: H II S2 S2 H II HST: S2 S1 S2 mini-BALQSO

4. F05189-2524 red Very Highly Ionized! F05189-2524 blue F05189-2524 UV

5. Search for Obscured QSOs with CXO/XMM  Trends with IRAS f 25 /f 60 color  Evidence for hidden QSOs in a few sources (also: Ptak et al. 2003; Franceschini et al. 2003) (Teng, Wilson, SV, Young, Sanders, & Nagar 2005) “cool” f 25 /f 60  “warm” L 2 – 10 keV /L FIR *burst AGN ULIRGs

6. NIR Spectroscopy  NIR signatures of AGN in most Seyfert ULIRGs, but not in LINER or HII ULIRGs (also Goldader+95, Murphy+01a, Lutz+02, and spectropolarimetry…)  L(BLR) / L(BOL): most ULIRGs with BLR are AGN-dominated (SV, Sanders, & Kim 1997, 1999)

7. ISO Spectroscopy (Tran et al. 2001) AGN *burst  Excellent agreement between optical/NIR and ISO classifications (e.g., Genzel et al. 1998; Lutz et al. 1999; Rigopoulou et al. 1999; Lutz, SV, & Genzel 1999; Tran et al. 2001)

8. QUEST: Quasar/ULIRG Evolutionary STudy  Medium-size Cycle-1 Spitzer program (95.3 hrs) Maryland: S. Veilleux (PI), D.-C. Kim, D. Rupke, A. Baker MPE: R. Genzel (co-PI), E. Sturm (Project Scientist), D. Lutz, …….. L. Tacconi, M. Lehnert, A. Contursi, K. Dasyra, M. Schweitzer Hawaii: D. Sanders, J. Barnes, R. Joseph, A. Stockton, O. Guyon IPAC: J. Mazzarella, S. Lord Tel Aviv U.: H. Netzer, A. Sternberg CWRU: C. Mihos

9. QUEST: Quasar/ULIRG Evolutionary STudy  Sample: 29 1-Jy ULIRGs + 25 PG QSOs Z < 0.3 This set of objects samples the full range of infrared luminosity and colors, merger state, and AGN/starburst fraction  SST Data Infrared Spectrograph (IRS) Low-resolution spectra: 5 – 14  m (SL2, SL1) High-resolution spectra: 10 – 37  m (SH, LH) High S/N

10. QUEST: Quasar/ULIRG Evolutionary STudy  Ancillary Data Optical & NIR ground-based imaging (Veilleux, Kim, Guyon, Sanders) NIR HST/NICMOS imaging (PI: Veilleux) NIR VLT spectroscopy (PI: Tacconi)  Evolutionary stage of the merger  Structure and dynamics of ULIRG progenitors  Structure and dynamics of ULIRG and QSO hosts  Locations of ULIRGs and QSOs in the fundamental plane of ellipticals SST/IRS spectra of optically- and infrared-selected LINERs (PI: Sturm)

11. Silicate Emissions in AGN: From LINERs to QSOs (Sturm et al. 2005; see also Hao et al. 2005; Siebenmorgen et al. 2005) AGN *burst  Signature of dust “obscuring torus” viewed face-on?  But: T dust ~ 200 K << T(torus walls) Not all Type 1 objects show silicate emission features  QSOs vs LINERs: dust composition? Grain size? Crystallization?

12. Hosts of Local ULIRGs  R and K´ images of 118 ULIRGs in 1-Jy sample (SV, Kim, & Sanders 2002)  Most of the 1-Jy sources are in the late stages of a merger  Remnants are often elliptical-like RK′K′ 1-Jy Sample

13. Low Surface Brightness Features  Signs of mergers visible in all ULIRGs and PG QSOs  Large-scale stellar disks visible in some systems (SV, Kim, Peng, Ho, et al. 2005) Data n=1 n = 4 UUQQUUQQ Deep HST H-band Imaging.  27 1-Jy ULIRGs.  6 PG QSOs

14. GALFIT Analysis: PSF + Sérsic component (SV, Kim, Peng, Ho, et al. 2005) n = 3.96 n = 1.0 n = 4.0

15. Low Surface Brightness Disks in ULIRGs and PG QSOs  Bulge + Disk in 3 objects  Lobsided or tidally- shredded “disks” in possibly 5 additional objects (SV, et al. 2005) Data Residuals Disk Bulge

16. Unsuspected Binaries  M…. (SV, et al. 2005)

17. Trends between Dominant Morphological Types, Spectral Types, and Infrared Colors  M…. (SV, et al. 2005)

18. Strength of tidal features  Strength of tidal features Tidal features are weaker among warm, AGN-like, early-type systems (SV, et al. 2005)

19. Sizes and Magnitudes of ULIRG & PG QSO Hosts ~ 2.7 kpc ~ (1.5 ± 1) L H * (SV, et al. 2005)

20. Photometric Fundamental Plane ULIRG & PG QSOs: Intermediate-mass ( ~ 1-2 m*) elliptical / lenticular galaxies. (consistent with Genzel et al. 2001; Tacconi et al. 2002; Dasyra et al. 2005) (SV, et al. 2005)

21. Environments of 1  Jy ULIRGs  B gc  Cluster-Galaxy correlation amplitude (e.g., Longair & Seldner 1979; Yee & López-Cruz 1999)  = 95 ± 16 Mpc 1.77  No obvious dependence on spectral type (Zauderer, SV, & Yee 2005 in prep) 0 1 2 ARC 3 * Starbursts ∙ LINERs ▲ Seyfert 2s ∙ Seyfert 1s

22. Environments of 1  Jy ULIRGs  Red = 1  Jy ULIRGs  Blue = RQ QSOs + RL QSOs + RGs (McLure & Dunlop 2001) (cf. Tacconi et al. 2002) (Zauderer, SV, & Yee 2005) 0 1 2 4 3

23. Environments of 1  Jy ULIRGs  Red = 1-Jy ULIRGs  Black = Seyferts (de Robertis et al. 1998) (Zauderer, SV, & Yee 2005)

24. Galactic Winds (Rupke, SV, & Sanders ‘02, ’05ab; also Martin 05) NGC 3079 HST + CXO % NGC 1482 [N II] / H  (Cecil, Bland-Hawthorn, & SV 2002 ) (SV & Rupke 2002 ) Blueshifted Na ID absorption lines (78 starbursts) (SV, Cecil, & Bland-Hawthorn 2005, ARAA; astro-ph/0504435)

25. Galactic Winds (Rupke, SV, & Sanders ‘02, ’05ab) NGC 3079 HST + CXO NGC 1482 [N II] / H  (Cecil, Bland-Hawthorn, & SV 2002 ) (SV & Rupke 2002 ) Blueshifted Na ID absorption lines (78 starbursts) (SV, Cecil, & Bland-Hawthorn 2005, ARAA; astro-ph/0504435) Na ID

26. Neutral Winds in Nearby LIRGs log (L IR ) ~ Starbursts Seyfert 2s Seyfert 1s Dwarfs (SM04) (Rupke, SV, & Sanders 2005abc) 80% Starburst99 30% Starburst99

27. Neutral Winds in Nearby LIRGs log (L IR ) ~ Starbursts Seyfert 2s Seyfert 1s Dwarfs (SM04) (Rupke, SV, & Sanders 2005abc) 80% Starburst99 30% Starburst99

28. Summary  AGN activity is present (and often dominant) in: > 30% of all local ULIRGs > 50% of local ULIRGs with log[L IR /L sun ] > 12.3 Stay tuned for upcoming SST results…  Hosts: Warm AGN-like systems have  prominent spheroids  weaker tidal features and stronger nuclei than cool LINER / HII systems  They are in the final phase of a merger The luminosities, sizes, and stellar masses of PG QSO hosts coincide with those of E-like 1-Jy ULIRGs  Environments: (preliminary) 1-Jy ULIRGs live in low-density environments although there are exceptions Good but not perfect overlap with environments of local Seyferts and QSOs  Galactic Winds: Winds are present in virtually all ULIRGs,, and are very significant and probably affect evolution

29. Summary  AGN activity is present (and often dominant) in: > 30% of all local ULIRGs > 50% of local ULIRGs with log[L IR /L sun ] > 12.3 Stay tuned for upcoming SST results…  Hosts: Warm AGN-like systems have  prominent spheroids  weaker tidal features and stronger nuclei than cool LINER / HII systems  They are in the final phase of a merger The luminosities, sizes, and stellar masses of PG QSO hosts coincide with those of E-like 1-Jy ULIRGs  Environments: (preliminary) 1-Jy ULIRGs live in low-density environments although there are exceptions Good but not perfect overlap with environments of local Seyferts and QSOs  Galactic Winds: Winds are present in virtually all ULIRGs,, and are very significant and probably affect evolution (SV, 08/15/05)